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CHIME All-sky Multiday Pulsar Stacking Search (CHAMPSS): System Overview and First Discoveries

T0 review · 2 major / 7 minor · reviewed 2026-08-16 · deepseek-v4-flash

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Pith's one-line read Stacking daily sky scans yields 11 new pulsars

desk verdict A solid, honest commissioning paper: the 11 new pulsars are real, the survey architecture is genuinely new, and the only place I would push back is the unquoted S600 flux calibration before trusting the 0.1 mJy floor. read the letter →

arxiv 2504.16293 v2 pith:53NOP4ZJ submitted 2025-04-22 astro-ph.HE

The CHAMPSS Collaboration , Christopher Andrade , P. J. Boyle , Charanjot Brar , Alyssa Cassity , Kathryn Crowter , Davor Cubranic , Abigail K. Denney
show 23 more authors
Fengqiu Adam Dong Emmanuel Fonseca Ajay Kumar Lars Künkel Magnus L'Argent Dustin Lang Robert A. Main Kiyoshi W. Masui Sujay Mate Juan Mena-Parra Bradley W. Meyers Cherry Ng Aaron B. Pearlman Ue-Li Pen Scott M. Ransom Alexander P. Roman Kendrick Smith Reynier Squillace Ingrid Stairs Chia Min Tan Laurent Tarabout Xia Wenke Tarik J. Zegmott
This is my paper · ORCID
classification astro-ph.HE
keywords pulsarsurveysradioastronomypowerspectrumstackingCHIMEdispersionmeasureneutronstarsfastFouriertransformall-skysurvey
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

CHAMPSS is a new way of searching for pulsars with a radio telescope that already watches most of the northern sky every day. Instead of using the telescope's fixed beams as single snapshots, the survey stitches adjacent beams into quasi-tracking beams, dedisperses each pointing to a sky-position-dependent maximum dispersion measure, and converts each observation into a power spectrum. Repeated visits to the same point on the sky are added together incoherently, so a pulsar too faint to show up in any one day can accumulate signal over weeks or months, while intermittent sources can be caught on days when they happen to pulse. In a commissioning survey covering about 6% of the sky over roughly two months, the pipeline found eleven previously unknown isolated pulsars with spin periods between 0.24 and 1.46 seconds and estimated flux densities between 0.24 and 0.89 mJy at 600 MHz. If the survey scales as planned to the full northern sky with more than a year of stacking per sightline, it reaches $\lesssim 30\,\mu$Jy sensitivity and becomes the deepest all-sky pulsar survey to date.

What carries the argument

The load-bearing mechanism is the power-spectrum stack. Each pointing's dedispersed time series is Fourier transformed, the resulting power spectra are barycentrically corrected, red-noise corrected, cleaned of radio-frequency interference using the zero-dispersion-measure spectrum as a reference, and then incoherently summed across days. Because the summed noise follows a $\chi^2_{2m}$ distribution, the significance of a real periodic signal grows as more days are added while noise fluctuations average down; harmonic summing over 1, 2, 4, 8, 16, and 32 harmonics collects power from narrow pulse profiles. A second mechanism is the pointing map, which sets the maximum searched dispersion measure from the larger of two Galactic electron models for each sightline and uses that limit to decide how finely to channelize the data, keeping the daily data volume manageable at 52 TB per day.

What would settle it

Re-observe the eleven pulsars with an independently calibrated telescope at 600 MHz and compare the measured flux densities with the values in the paper's table; a systematic offset larger than a factor of two in the same direction would falsify the quantitative sensitivity claim, as would showing that the weakest pulsar, J2302+4807, falls below 0.1 mJy under a re-derived calibration.

Watch

Extended reading notes

Core claim

The central discovery is that a survey built on the daily, all-sky intensity stream of a transit radio telescope can discover pulsars by combining stationary beams into quasi-tracking beams, dedispersing to position-dependent dispersion-measure limits, and summing power spectra across many days. The eleven new pulsars demonstrate the concept: all were confirmed by folding, six of them have fitted timing solutions, and their periods, dispersion measures, and flux densities are tabulated. Three of the pulsars have dispersion measures above what standard Galactic electron models predict for their sightlines, which the paper interprets as evidence that the survey will reveal where those models fail. The intended endpoint is a full northern-sky survey that stacks more than a year of data per pointing and reaches $\lesssim 30\,\mu$Jy, which the paper argues will make it deeper than any previous all-sky pulsar survey.

Load-bearing premise

The reported flux-density range depends on converting uncalibrated pulse profiles into janskys using the telescope's noise temperature measured from calibrator radio sources; if that calibration carries a systematic error larger than roughly a factor of two, some of the reported values could drop below the 0.1 mJy lower bound stated in the abstract, although the existence of the eleven pulsars themselves does not depend on this calibration.

Editorial extensions

If this is right

  • The full survey, stacking more than one year per pointing, reaches $\lesssim 30\,\mu$Jy for all sightlines above a declination of $10^\circ$ and away from the Galactic plane, making it the deepest all-sky pulsar survey.
  • Daily repeated observations give the survey sensitivity to intermittent pulsars—nulling, eclipsing, scintillating, or precessing sources—that single-visit surveys can miss.
  • New pulsars on under-searched sightlines, especially those with dispersion measures in excess of model predictions, will help refine Galactic electron density models and clarify the boundary between high-dispersion-measure Galactic pulsars and low-dispersion-measure fast radio bursts.
  • The survey is complementary to targeted coherent follow-up observations: CHAMPSS finds faint candidates in the power-spectrum stack, and the follow-up timing pipeline converts them into pulsars with measured positions, spin periods, and period derivatives.
  • The eleven commissioning discoveries, confirmed by folding and partly by timing solutions, show that the full pipeline from data acquisition to candidate confirmation works end to end.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The same stacking design could be transferred to other large-format, transit-style radio arrays, turning fixed beams into effective tracking surveys at a fraction of the data rate of tied-array beamforming.
  • If the flux-density calibration holds up, the survey's per-pointing depth will keep growing with the square root of the number of stacked days, so the final sensitivity will depend on maintaining stable radio-frequency-interference statistics and calibration over years.
  • The three dispersion-measure-excess pulsars hint that the survey will double as a wide-field probe of Galactic ionized structures such as H II regions, potentially tracing their geometry through many new pulsar sightlines.
  • A testable extension would be to run the same power-spectrum stacking and clustering machinery on shorter time intervals, which could catch weakly periodic sources that are not stable enough to appear in month-long stacks.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 7 minor

Summary. The paper presents CHAMPSS, a pulsar periodicity search built on the CHIME/FRB intensity datastream. It describes the formation of quasi-tracking beams from adjacent static beams, position-dependent dedispersion and DM limits, power-spectrum generation, incoherent stacking over many days, candidate clustering, and follow-up via folding and timing. In a commissioning survey covering roughly 6% of the northern sky, the pipeline discovered 11 previously unknown isolated pulsars with spin periods 0.24-1.46 s and estimated S600 flux densities of 0.24-0.89 mJy, all confirmed by folded profiles and presented with timing residuals. The paper also validates the sensitivity model against known pulsars and reports three new pulsars with DMs in excess of NE2001/YMW16 predictions, including a scattered pulsar near the Cygnus region.

Significance. If the quantitative flux scale is confirmed, this is an important result: CHAMPSS demonstrates a new survey mode that revisits the full northern sky daily and reaches faint flux densities by incoherently stacking power spectra, with a real-time pipeline and a public codebase. The core discovery claim is credible because candidates were confirmed by folding and timing rather than by the search statistic alone, and the DM-excess pulsars provide falsifiable input for Galactic electron models. The paper's main weakness is the absolute calibration of the S600 values, which carries no quoted uncertainties and is load-bearing for the abstract's flux floor. The forecast sensitivity of the full survey is plausible but not yet demonstrated.

major comments (2)
  1. [§6.1, Eq. (8), Table 1] The S600 values are load-bearing for the abstract claim that all eleven new pulsars have S600 > 0.1 mJy and for the flux column of Table 1, but they are derived from uncalibrated CHIME/Pulsar profiles under two unchecked assumptions: that the off-pulse mean of the profile equals the SEFD and that a single frequency-averaged SEFD is representative across 400-800 MHz. No uncertainties are quoted for any S600 value, and the faintest source (J2302+4807, 0.24 mJy) is only a factor of 2.4 above the 0.1 mJy threshold. A correlated calibration error of order 2-3x would therefore invalidate the abstract's flux floor and change the reported range, even though it would not affect the existence of the discoveries. Please provide a systematic error budget for Eq. (8), validate the SEFD assumptions with data, or soften the abstract and table claims to explicitly reflect the calibration uncertainty.
  2. [§6.1, Table 1, Fig. 20] The text states that only 6 of the 11 pulsars have sufficient follow-up observations to derive timing solutions, yet Table 1 lists spin period and period-derivative values with uncertainties for all 11 pulsars and Figure 20 shows timing residuals for all 11. Please reconcile this inconsistency: either all 11 pulsars are phase-connected and timed, in which case the '6' is incorrect, or only 6 are, in which case the table and residual figure overstate the confirmation status. This matters because the paper's central claim is that all eleven sources are confirmed pulsars.
minor comments (7)
  1. [Figure 14 and Table 1] The pulsar labeled 'J2118+5001' in Figure 14 does not match 'J2118+5143' in Table 1; please correct the figure or the table.
  2. [Abstract and §6] The abstract says the commissioning data were searched 'over two months', while §6 describes a realtime survey running from October 2023 to June 2024 with each beamrow recorded for over a month; please clarify whether 'two months' refers to the stacking interval rather than the survey duration.
  3. [§2.1 and §3.2] The time resolution is given as 0.98304 ms, 0.98306 ms, and 0.983 ms in different places; please use a single consistent value.
  4. [§4.2, Eq. (4)] Equation (4) is typeset incorrectly in the text ('f t 1≈'); it should read phi(t) = f0 t1 + (1/2) fdot t1^2, with t1 = t - tref.
  5. [§6.2, Fig. 15] The 'good agreement' between predicted and detected S/N would be easier to assess if the plot included the number of known pulsars used and a quantitative measure of scatter or bias; as presented, the plot alone is not fully sufficient to validate the sensitivity model.
  6. [§3.9] The 5-sigma and 6-sigma thresholds are quoted without a discussion of the number of independent trials; a sentence quantifying the effective trial factor and resulting false-positive rate would make the candidate filtering description more complete.
  7. [§8.1] In the candidate plot description, 'O Text Text field' appears to be a typo; it should read 'O Text field'.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity found: the discoveries are empirical detections confirmed by folding and timing, and the sensitivity/flux claims rest on independently calibrated and externally benchmarked quantities.

full rationale

The paper's central claim is the detection of eleven previously unknown pulsars through a periodicity search of CHIME/FRB intensity data, followed by confirmation via folding, multiday phase-connecting searches, and timing. None of these steps defines the detection threshold or the candidate significance in terms of the discovered pulsars themselves. The flux densities in Table 1 are derived using Eq. 8 from uncalibrated CHIME/Pulsar profiles scaled by SEFD values obtained from calibrator sources monitored independently by CHIME/Pulsar; the SEFD is not fitted to the newly discovered pulsars, so the S600 values are calibrated measurements rather than predictions forced by an input. The survey sensitivity model in Section 6.2 uses the radiometer equation with independently adopted receiver temperature, sky temperature model, gain, and catalogued flux densities of known pulsars from ATNF, comparing predicted S/N with measured S/N; this is an external benchmark, not a self-referential fit. DM search ranges are set from NE2001 and YMW16 Galactic electron models, and three pulsars are found with DM in excess of the models, which contradicts rather than presupposes those inputs. The paper's self-citations are descriptive references to CHIME/FRB and CHIME/Pulsar instrument papers and calibration methods; they are not load-bearing mathematical reductions and do not import an unverified uniqueness claim or ansatz. The only notable uncertainty is the absolute flux calibration scale in Eq. 8, which could affect the quantitative S600 floor if systematic errors exceed a factor of about two, but this is a measurement-calibration risk, not circularity: the existence and periods of the pulsars do not depend on it. Accordingly, the appropriate circularity score is 0.

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The central claims are empirical; the only hand-chosen numbers are survey-design choices such as the DM search margin and detection thresholds, which affect completeness and sensitivity estimates rather than the existence of the 11 pulsars. No new physical entities are introduced.

free parameters (2)
  • DM search margin heuristic coefficients = 0.0313 and 0.223 in exp(0.0313|gb| + 0.223)
    Chosen by hand in Section 3.3 to make the searched DM range rise from 1.25 times the model maximum at the Galactic plane to 2.0 times at |gb| = 15 degrees. This affects survey completeness but not the existence of the discovered pulsars.
  • Detection significance thresholds = 5 sigma for daily searches, 6 sigma for stacked searches
    Hand-set thresholds in Section 3.9 that define which power-spectrum peaks become detections and feed the clustering and confirmation chain. They are standard choices rather than fitted constants.
assumptions (5)
  • standard math Power spectra of pure Gaussian noise follow a chi-squared distribution with 2m degrees of freedom when m powers are summed.
    Used in Eq. (1) and Section 3.9 to convert summed harmonic powers and stacked powers into Gaussian-equivalent significances for detections.
  • domain assumption The radiometer equation with the stated gain, receiver temperature, sky model, and bandwidth predicts the minimum detectable flux density for pulsars.
    Section 6.2 uses this equation to compare predicted and detected signal-to-noise ratios for known pulsars and to project the 30 microjansky full-survey sensitivity.
  • domain assumption The NE2001 and YMW16 Galactic electron models, combined with the heuristic margin, give adequate upper bounds on the DM of Galactic pulsars for setting search ranges.
    Section 3.3 sets DMsearch from these models; the paper's own discovery of three pulsars with DM in excess of one or both models shows this assumption is imperfect, though not violated for the discovered sources.
  • domain assumption The 3-bit Huffman-coded downsampling of the CHIME/FRB datastream preserves the periodic signals with roughly 5 percent information loss.
    Described in Section 3.2; the commissioning discoveries support this for the actual sources, but the full-survey sensitivity projections assume it continues to hold.
  • domain assumption Barycentric correction in the power-spectrum domain using nearest-neighbor interpolation is sufficient to align power spectra from different days.
    Section 3.6 relies on this to enable incoherent stacking; small interpolation errors would smear frequency bins but the successful stacked detections suggest the effect is manageable.

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Cite this review

Pith. "Pith review of CHIME All-sky Multiday Pulsar Stacking Search (CHAMPSS): System Overview and First Discoveries." pith.science (2026). https://pith.science/paper/53NOP4ZJ

@misc{pith2026250416293,
  author       = {Pith},
  title        = {Pith review of: CHIME All-sky Multiday Pulsar Stacking Search (CHAMPSS): System Overview and First Discoveries},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/53NOP4ZJ}},
  note         = {Machine review of arXiv:2504.16293}
}
abstract

We describe the CHIME All-sky Multiday Pulsar Stacking Search (CHAMPSS) project. This novel radio pulsar survey revisits the full Northern Sky daily, offering unprecedented opportunity to detect highly intermittent pulsars, as well as faint sources via long-term data stacking. CHAMPSS uses the CHIME/FRB datastream, which consists of 1024 stationary beams streaming intensity data at $0.983$\,ms resolution, 16384 frequency channels across 400--800\,MHz, continuously being searched for single, dispersed bursts/pulses. In CHAMPSS, data from adjacent east-west beams are combined to form a grid of tracking beams, allowing longer exposures at fixed positions. These tracking beams are dedispersed to many trial dispersion measures (DM) to a maximum DM beyond the Milky Way's expected contribution, and Fourier transformed in time to form power spectra. Repeated observations are searched daily to find intermittent sources, and power spectra of the same sky positions are incoherently stacked, increasing sensitivity to faint persistent sources. The $0.983$\,ms time resolution limits our sensitivity to millisecond pulsars; we have full sensitivity to pulsars with $P > 60\,$ms, with sensitivity gradually decreasing from $60$ ms to $2$\,ms as higher harmonics are beyond the Nyquist limit. In a commissioning survey, data covering $\sim 1/16$ of the CHIME sky was processed and searched in quasi-realtime over two months, leading to the discovery of eleven new pulsars, each with $S_{600} > 0.1$\,mJy. When operating at scale, CHAMPSS will stack $>$1\,year of data along each sightline, reaching a sensitivity of $\lesssim 30\, \mu$Jy for all sightlines above a declination of $10^{\circ}$, and off of the Galactic plane.

Figures

Figures reproduced from arXiv: 2504.16293 by the authors.

Figure 1
Figure 1. Simplified flowchart of the CHAMPSS pipeline, as described in Sections 3, 4. The dotted arrow to the Machine Learning candidate classifier indicates that it is a planned component of our pipeline, which was not used in our commissioning survey. ever copy long-term data products to a supercomputing cluster ‘Narval’, owned and operated by Calcul Québec, where we have a 2.2 PB storage allocation. The timing pipeline (S… view at source ↗
Figure 2
Figure 2. CHAMPSS pointing map. The color bar represents the maximum DM that we search to along a given sightline in units of pc cm−3 . The contours indicate increasing number of channels in powers of 2, representing 5 tiers from 1024 to 16384. The grey shaded region denotes our commissioning survey, the orange stars denote the newly discovered pulsars, and the magenta points show known pulsars which our survey detected. 0 20… view at source ↗
Figure 3
Figure 3. Duration (top) and sensitivity (bottom) of point￾ings as a function of declination. Pointings at high-dec di￾verge in time as sources spend longer in the beam; pointings longer than 2 22 samples ≈ 68.7 min are split, for memory lim￾itations. A linear fit to these windowed median values then pro￾vides a local red-noise estimate for each frequency bin, which is divided into the data value. Two schemes for RFI suppress… view at source ↗
Figures from the paper (17 more)
Figure 4
Figure 4. Figure 4: Candidate significance for four of our new pulsars as a function of number of days stacked. The horizontal black line shows the threshold of 6σ which we currently use during the stack searching process. In this run a threshold of 5σ was used and the stack was searched …
Figure 5
Figure 5. Figure 5: Example showing bins in a power spectrum shared by a 32 harmonic sum for a detection at f (high￾lighted in red) and a 8 harmonic sum for a detection at 13f /3 (blue). DM of 2 pc cm−3 are filtered. Additionally, all clusters which have a mean frequency within the freque…
Figure 6
Figure 6. Figure 6: Candidate plot for a detection of our new pul￾sar PSR J2108+5001 in a single observation. The various diagnostic plots show how the signal develops as a function of frequency and DM. It also shows the signal strength at various harmonic frequencies. The clustered detec…
Figure 7
Figure 7. Figure 7: Example of a pulsar (left), and RFI candidate (right). The plots are the result of the multi-pointing clustering process. The upper parts of the plots the show the data of strongest clustered detections and the lower part of the plots show information derived from the …
Figure 8
Figure 8. Figure 8: Example of a candidate plot for a single-day fold, on newly discovered pulsar PSR J2319+4919. The side panels are akin to PRESTO plots, showing the χ 2 as a function of f and ˙f (top), and I(ϕ, DM) (bottom). The top contains information of the candidate leading to the …
Figure 9
Figure 9. Figure 9: An example of our multiday search script for candidate confirmation, which searches a grid of f, ˙f values as described in Section 4.2. All of our newly discovered pul￾sars were found with high significance from this algorithm. Shown above is known pulsar PSR J2208+461…
Figure 10
Figure 10. Figure 10: An example output from the timing pipeline described in Section 4.3 with PSR J2100+4711. Left: Pulse intensity (greyscale) as a function of phase and date of pulse profiles after the timing model has been applied (bottom), and their stacked profile by summing over tim…
Figure 11
Figure 11. Figure 11: LST-averaged residuals for aliased timing so￾lutions for J2108+5001. For each line, the frequency in the timing solution was adjusted by nfsid, TOAs were then re￾fitted, and residuals at similar local sidereal times were av￾eraged together. A slope indicates residuals…
Figure 12
Figure 12. Figure 12: (Top:) Varying period found from the single-day candidate folds of PSR B2303+46, in an eccentric (e = 0.658) 12.34 day orbit. The pulsar was treated as an unknown can￾didate, folded with a constant period from the peak of f in the stack, and folded daily using the sta…
Figure 13
Figure 13. Figure 13: Example data visualization for a given day’s data product. Orange points represent known pulsars from the PSRCAT database, purple and pink points are multi￾pointing candidates from the pipeline, red points are candi￾dates that were associated with a known source. The …
Figure 14
Figure 14. Figure 14: Panorama of newly discovered pulsars. The pulsars have been averaged in frequency across the band, binned to 128 phase bins, and averaged over 10 days. for which we use calibrator radio sources monitored by CHIME/Pulsar, as outlined in Section 3.5 of Dong (2024). Meas…
Figure 15
Figure 15. Figure 15: Comparison of expected vs. actual signal-to￾noise values for folded known pulsars that lie within the CHAMPSS commissioning survey RA/Dec range. An up￾per limit is indicated for pulsars that are not detected by CHAMPSS and the dashed line is the line of equality. We c…
Figure 16
Figure 16. Figure 16: Ratio of the new discovered pulsar’s DM to the maximum from NE2001, YMW16, and the max search DM from our pointing map. Although Galactic, three pulsars are in excess of NE2001 and/or YMW16, indicating a higher DM than predicted for the entire Milky Way. Despite the e…
Figure 17
Figure 17. Figure 17: Fitburst (Fonseca et al. 2024) modelling of the pulse profile for PSR J2108+5001. The central plot shows the model, with the data to the left and residuals to the right. and in a commissioning survey covering ≈ 6% of the sky over 2 months, we discovered 11 new pulsars…
Figure 18
Figure 18. Figure 18: Excess DM beyond the Galactic maxi￾mum predicted by the YMW16 model in the vicinity of PSR J2108+5001. Pulsars with DMs within model predic￾tions are not shown and PSR J2108+5001 is highlighted with a black ring. Contours show the Finkbeiner (2003) Hα map at values of…
Figure 19
Figure 19. Figure 19: Example multi-pointing candidate plot of PSR J2047+5029. Red alphabetic labels have been added to the individual segments of the plot. 8. APPENDIX 8.1. Description of Candidate Plots [PITH_FULL_IMAGE:figures/full_fig_p024_19.png]
Figure 20
Figure 20. Figure 20: Timing residuals for 11 newly discovered pulsars. Pulsar names (top), periods, and reduced χ 2 (bottom) of the fit are given to the left of each plot. Black, blue, and red data points are residuals (with their errorbars) of TOAs from CHAMPSS, CHIME/Pulsar fold-mode, a…

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Reference graph

Works this paper leans on

77 extracted references · 6 canonical work pages

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    The CHIME Fast Radio Burst Project: System Overview

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

    arXiv 2021

  4. [4]

    2020, ACM Trans

    Abergel, R., & Moisan, L. 2020, ACM Trans. Math. Softw., 46, 10:1, 10.1145/3365983

    work page doi:10.1145/3365983 2020

  5. [5]

    M., et al

    Agazie , G., Anumarlapudi , A., Archibald , A. M., et al. 2023, , 951, L8, 10.3847/2041-8213/acdac6

    doi:10.3847/2041-8213/acdac6 2023

  6. [6]

    D., Bania, T

    Anderson, L. D., Bania, T. M., Balser, D. S., et al. 2014, The Astrophysical Journal Supplement Series, 212, 1, 10.1088/0067-0049/212/1/1

    doi:10.1088/0067-0049/212/1/1 2014

  7. [7]

    Anderson , S. B. 1993, PhD thesis, California Institute of Technology

    work page 1993

  8. [8]

    Backer , D. C. 1970, , 228, 42, 10.1038/228042a0

    doi:10.1038/228042a0 1970

Show all 77 references
  1. [9]

    C., Kulkarni , S

    Backer , D. C., Kulkarni , S. R., Heiles , C., Davis , M. M., & Goss , W. M. 1982, , 300, 615, 10.1038/300615a0

    1982 doi

  2. [10]

    Bhat , N. D. R., Swainston , N. A., McSweeney , S. J., et al. 2023 a , , 40, e021, 10.1017/pasa.2023.17

    2023 doi

  3. [11]

    2023 b , , 40, e020, 10.1017/pasa.2023.18

    ---. 2023 b , , 40, e020, 10.1017/pasa.2023.18

    2023 doi

  4. [12]

    P., Kaspi , V

    Breton , R. P., Kaspi , V. M., Kramer , M., et al. 2008, Science, 321, 104, 10.1126/science.1159295

    2008 doi

  5. [13]

    M., Freire , P

    Cadelano , M., Ransom , S. M., Freire , P. C. C., et al. 2018, , 855, 125, 10.3847/1538-4357/aaac2a

    2018 doi

  6. [14]

    2022, , 261, 29, 10.3847/1538-4365/ac6fd9

    CHIME Collaboration , Amiri , M., Bandura , K., et al. 2022, , 261, 29, 10.3847/1538-4365/ac6fd9

    2022 doi

  7. [15]

    2018, , 863, 48, 10.3847/1538-4357/aad188

    CHIME/FRB Collaboration , Amiri , M., Bandura , K., et al. 2018, , 863, 48, 10.3847/1538-4357/aad188

    2018 doi

  8. [16]

    C., et al

    CHIME/FRB Collaboration , Amiri , M., Andersen , B. C., et al. 2021, , 257, 59, 10.3847/1538-4365/ac33ab

    2021 doi

  9. [17]

    M., et al

    CHIME/Pulsar Collaboration , Amiri , M., Bandura , K. M., et al. 2021, , 255, 5, 10.3847/1538-4365/abfdcb

    2021 doi

  10. [18]

    M., Bhardwaj , M., Gaensler , B

    Cook , A. M., Bhardwaj , M., Gaensler , B. M., et al. 2023, , 946, 58, 10.3847/1538-4357/acbbd0

    2023 doi

  11. [19]

    M., & Lazio , T

    Cordes , J. M., & Lazio , T. J. W. 2002, arXiv e-prints, astro, 10.48550/arXiv.astro-ph/0207156

    2002 doi arXiv

  12. [20]

    B., Pennucci , T., Ransom , S

    Demorest , P. B., Pennucci , T., Ransom , S. M., Roberts , M. S. E., & Hessels , J. W. T. 2010, , 467, 1081, 10.1038/nature09466

    2010 doi

  13. [21]

    2024, PhD thesis, University of British Columbia, http://dx.doi.org/10.14288/1.0445624

    Dong, F. 2024, PhD thesis, University of British Columbia, http://dx.doi.org/10.14288/1.0445624

    2024 doi

  14. [22]

    A., Crowter , K., Meyers , B

    Dong , F. A., Crowter , K., Meyers , B. W., et al. 2023, , 524, 5132, 10.1093/mnras/stad2012

    2023 doi

  15. [23]

    2023, , 678, A50, 10.1051/0004-6361/202346844

    EPTA Collaboration , InPTA Collaboration , Antoniadis , J., et al. 2023, , 678, A50, 10.1051/0004-6361/202346844

    2023 doi

  16. [24]

    Finkbeiner, D. P. 2003, The Astrophysical Journal Supplement Series, 146, 407, 10.1086/374411

    2003 doi

  17. [25]

    M., Williams , J

    Folkner , W. M., Williams , J. G., & Boggs , D. H. 2009, Interplanetary Network Progress Report, 42-178, 1

    2009

  18. [26]

    T., Pennucci , T

    Fonseca , E., Cromartie , H. T., Pennucci , T. T., et al. 2021, , 915, L12, 10.3847/2041-8213/ac03b8

    2021 doi

  19. [27]

    2024, , 271, 49, 10.3847/1538-4365/ad27d6

    Fonseca , E., Pleunis , Z., Breitman , D., et al. 2024, , 271, 49, 10.3847/1538-4365/ad27d6

    2024 doi

  20. [28]

    S., Stinebring , D

    Fruchter , A. S., Stinebring , D. R., & Taylor , J. H. 1988, , 333, 237, 10.1038/333237a0

    1988 doi

  21. [29]

    C., Andersen , B

    Good , D. C., Andersen , B. C., Chawla , P., et al. 2021, , 922, 43, 10.3847/1538-4357/ac1da6

    2021 doi

  22. [30]

    L., Manchester , R

    Han , J. L., Manchester , R. N., Lyne , A. G., Qiao , G. J., & van Straten , W. 2006, , 642, 868, 10.1086/501444

    2006 doi

  23. [31]

    L., Wang , C., Wang , P

    Han , J. L., Wang , C., Wang , P. F., et al. 2021, Research in Astronomy and Astrophysics, 21, 107, 10.1088/1674-4527/21/5/107

    2021 doi

  24. [32]

    L., Zhou , D

    Han , J. L., Zhou , D. J., Wang , C., et al. 2025, Research in Astronomy and Astrophysics, 25, 014001, 10.1088/1674-4527/ada3b7

    2025 doi

  25. [33]

    Haslam , C. G. T., Salter , C. J., Stoffel , H., & Wilson , W. E. 1982, , 47, 1

    1982

  26. [34]

    W., van Straten , W., & Manchester , R

    Hotan , A. W., van Straten , W., & Manchester , R. N. 2004, , 21, 302, 10.1071/AS04022

    2004 doi

  27. [35]

    Huffman, D. A. 1952, Proceedings of the IRE, 40, 1098, 10.1109/JRPROC.1952.273898

    1952

  28. [36]

    N., Lyne , A

    Johnston , S., Manchester , R. N., Lyne , A. G., et al. 1992, , 387, L37, 10.1086/186300

    1992 doi

  29. [37]

    Kaplan , D. L. 2022, PSS: Pulsar Survey Scraper , Astrophysics Source Code Library, record ascl:2210.001

    2022

  30. [38]

    H., Manchester , R

    Kramer , M., Stairs , I. H., Manchester , R. N., et al. 2021, Physical Review X, 11, 041050, 10.1103/PhysRevX.11.041050

    2021 doi

  31. [39]

    I., Vaughan , A

    Large , M. I., Vaughan , A. E., & Mills , B. Y. 1968, , 220, 340, 10.1038/220340a0

    1968 doi

  32. [40]

    M., & Prakash , M

    Lattimer , J. M., & Prakash , M. 2007, , 442, 109, 10.1016/j.physrep.2007.02.003

    2007 doi

  33. [41]

    2021, , 911, 45, 10.3847/1538-4357/abe62f

    Luo , J., Ransom , S., Demorest , P., et al. 2021, , 911, 45, 10.3847/1538-4357/abe62f

    2021 doi

  34. [42]

    2010, Science, 329, 408, 10.1126/science.1186683

    Lyne , A., Hobbs , G., Kramer , M., Stairs , I., & Stappers , B. 2010, Science, 329, 408, 10.1126/science.1186683

    2010 doi

  35. [43]

    N., Hobbs , G

    Manchester , R. N., Hobbs , G. B., Teoh , A., & Hobbs , M. 2005, , 129, 1993, 10.1086/428488

    2005 doi

  36. [44]

    N., Lyne , A

    Manchester , R. N., Lyne , A. G., Camilo , F., et al. 2001, , 328, 17, 10.1046/j.1365-8711.2001.04751.x

    2001

  37. [45]

    Massey, F. J. 1951, Journal of the American Statistical Association, 46, 68

    1951

  38. [46]

    P., Shin , K., et al

    Merryfield , M., Tendulkar , S. P., Shin , K., et al. 2023, , 165, 152, 10.3847/1538-3881/ac9ab5

    2023 doi

  39. [47]

    C., Lamb , F

    Miller , M. C., Lamb , F. K., Dittmann , A. J., et al. 2021, , 918, L28, 10.3847/2041-8213/ac089b

    2021 doi

  40. [48]

    D., Cooper , S., et al

    Morello , V., Barr , E. D., Cooper , S., et al. 2019, , 483, 3673, 10.1093/mnras/sty3328

    2019 doi

  41. [49]

    2017, in XXXII International Union of Radio Science General Assembly & Scientific Symposium (URSI GASS) 2017, 4, 10.23919/URSIGASS.2017.8105318

    Ng , C., Vanderlinde , K., Paradise , A., et al. 2017, in XXXII International Union of Radio Science General Assembly & Scientific Symposium (URSI GASS) 2017, 4, 10.23919/URSIGASS.2017.8105318

    2017

  42. [50]

    M., & Gary , D

    Nita , G. M., & Gary , D. E. 2010 a , , 406, L60, 10.1111/j.1745-3933.2010.00882.x

    2010

  43. [51]

    2010 b , , 122, 595, 10.1086/652409

    ---. 2010 b , , 122, 595, 10.1086/652409

    2010 doi

  44. [52]

    M., Gary, D

    Nita, G. M., Gary, D. E., & Hellbourg, G. 2016, in 2016 Radio Frequency Interference (RFI), 75--80, 10.1109/RFINT.2016.7833535

    2016

  45. [53]

    M., Hickish , J., MacMahon , D., & Gary , D

    Nita , G. M., Hickish , J., MacMahon , D., & Gary , D. E. 2016, Journal of Astronomical Instrumentation, 5, 1641009, 10.1142/S2251171716410099

    2016 doi

  46. [54]

    K., Anderson , L

    Ocker , S. K., Anderson , L. D., Lazio , T. J. W., Cordes , J. M., & Ravi , V. 2024, arXiv e-prints, arXiv:2406.07664, 10.48550/arXiv.2406.07664

    2024 doi arXiv

  47. [55]

    K., Cordes , J

    Ocker , S. K., Cordes , J. M., Chatterjee , S., & Gorsuch , M. R. 2022, , 934, 71, 10.3847/1538-4357/ac75ba

    2022 doi

  48. [56]

    V., Barr , E

    Padmanabh , P. V., Barr , E. D., Sridhar , S. S., et al. 2023, , 524, 1291, 10.1093/mnras/stad1900

    2023 doi

  49. [57]

    2016, , 459, L26, 10.1093/mnrasl/slw037

    Pan , Z., Hobbs , G., Li , D., et al. 2016, , 459, L26, 10.1093/mnrasl/slw037

    2016 doi

  50. [58]

    M., Ransom , S

    Parent , E., Kaspi , V. M., Ransom , S. M., et al. 2018, , 861, 44, 10.3847/1538-4357/aac5f0

    2018 doi

  51. [59]

    2010, Highlights of Astronomy, 15, 220, 10.1017/S1743921310008896

    Petit , G. 2010, Highlights of Astronomy, 15, 220, 10.1017/S1743921310008896

    2010 doi

  52. [60]

    2022, , 163, 84, 10.3847/1538-3881/ac403e

    Phillips , C., & Ransom , S. 2022, , 163, 84, 10.3847/1538-3881/ac403e

    2022 doi

  53. [61]

    2023, Monthly Notices of the Royal Astronomical Society, 520, 4582–4600, 10.1093/mnras/stac3383

    Posselt, B., Karastergiou, A., Johnston, S., et al. 2023, Monthly Notices of the Royal Astronomical Society, 520, 4582–4600, 10.1093/mnras/stac3383

    2023 doi

  54. [62]

    Price , D. C. 2021, Research Notes of the American Astronomical Society, 5, 246, 10.3847/2515-5172/ac332c

    2021 doi

  55. [63]

    2011, PRESTO: PulsaR Exploration and Search TOolkit , Astrophysics Source Code Library, record ascl:1107.017

    Ransom , S. 2011, PRESTO: PulsaR Exploration and Search TOolkit , Astrophysics Source Code Library, record ascl:1107.017

    2011

  56. [64]

    M., Eikenberry , S

    Ransom , S. M., Eikenberry , S. S., & Middleditch , J. 2002, , 124, 1788, 10.1086/342285

    2002 doi

  57. [65]

    J., Zic , A., Shannon , R

    Reardon , D. J., Zic , A., Shannon , R. M., et al. 2023, , 951, L6, 10.3847/2041-8213/acdd02

    2023 doi

  58. [66]

    Rickett , B. J. 1990, , 28, 561, 10.1146/annurev.aa.28.090190.003021

    1990

  59. [67]

    G., et al

    Sanidas , S., Cooper , S., Bassa , C. G., et al. 2019, , 626, A104, 10.1051/0004-6361/201935609

    2019 doi

  60. [68]

    A., Abdollahi , S., Ajello , M., et al

    Smith , D. A., Abdollahi , S., Ajello , M., et al. 2023, , 958, 191, 10.3847/1538-4357/acee67

    2023 doi

  61. [69]

    Staelin , D. H. 1969, IEEE Proceedings, 57, 724, 10.1109/PROC.1969.7051

    1969

  62. [70]

    H., & Reifenstein , III, E

    Staelin , D. H., & Reifenstein , III, E. C. 1968, Science, 162, 1481, 10.1126/science.162.3861.1481

    1968

  63. [71]

    R., Rickett , B

    Stinebring , D. R., Rickett , B. J., Minter , A. H., et al. 2022, , 941, 34, 10.3847/1538-4357/ac8ea8

    2022 doi

  64. [72]

    S., Ransom , S

    Stovall , K., Lynch , R. S., Ransom , S. M., et al. 2014, , 791, 67, 10.1088/0004-637X/791/1/67

    2014 doi

  65. [73]

    H., & Weisberg , J

    Taylor , J. H., & Weisberg , J. M. 1989, , 345, 434, 10.1086/167917

    1989 doi

  66. [74]

    1989, in NATO Advanced Study Institute (ASI) Series C, Vol

    van der Klis , M. 1989, in NATO Advanced Study Institute (ASI) Series C, Vol. 262, Timing Neutron Stars, ed. H. \"O gelman & E. P. J. van den Heuvel , 27, 10.1007/978-94-009-2273-0_3

    1989 doi

  67. [75]

    E., et al

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, Nature Methods, 17, 261, 10.1038/s41592-019-0686-2

    2020 doi

  68. [76]

    M., Manchester , R

    Yao , J. M., Manchester , R. N., & Wang , N. 2017, , 835, 29, 10.3847/1538-4357/835/1/29

    2017 doi

  69. [77]

    Zackay , B., & Ofek , E. O. 2017, , 835, 11, 10.3847/1538-4357/835/1/11

    2017 doi

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